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Start Over Author "Fouqué, P." Publisher american astronomical society
11 results on '"Fouqué, P."'

1. MOA-2016-BLG-227Lb: A Massive Planet Characterized by Combining Light-curve Analysis and Keck AO Imaging

Author

Koshimoto, N., Shvartzvald, Y., Bennett, D. P., Penny, M. T., Hundertmark, M., Bond, I. A., Zang, W. C., Henderson, C. B., Suzuki, D., Rattenbury, N. J., Sumi, T., Abe, F., Asakura, Y., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Tristram, P. J., Yamada, T., Yonehara, A., Gelino, C. R., Beichman, C., Beaulieu, J.-P., Marquette, J.-B., Batista, V., Friedmann, M., Hallakoun, N., Kaspi, S., Maoz, D., Bryden, G., Novati, S. Calchi, Howell, S. B., Wang, T. S., Mao, S., Fouqué, P., Korhonen, H., Jørgensen, U. G., Street, R., Tsapras, Y., Dominik, M., Kerins, E., Cassan, A., Snodgrass, C., Bachelet, E., Bozza, V., Bramich, D. M., University of St Andrews. St Andrews Centre for Exoplanet Science, and University of St Andrews. School of Physics and Astronomy

Subjects
Proper motion, NDAS, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 01 natural sciences, micro [Gravitational lensing], law.invention, Telescope, law, Planet, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy and Astrophysics, Mass ratio, Light curve, Planetary systems, Stars, QC Physics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of a microlensing planet --- MOA-2016-BLG-227Lb --- with a large planet/host mass ratio of $q \simeq 9 \times 10^{-3}$. This event was located near the $K2$ Campaign 9 field that was observed by a large number of telescopes. As a result, the event was in the microlensing survey area of a number of these telescopes, and this enabled good coverage of the planetary light curve signal. High angular resolution adaptive optics images from the Keck telescope reveal excess flux at the position of the source above the flux of the source star, as indicated by the light curve model. This excess flux could be due to the lens star, but it could also be due to a companion to the source or lens star, or even an unrelated star. We consider all these possibilities in a Bayesian analysis in the context of a standard Galactic model. Our analysis indicates that it is unlikely that a large fraction of the excess flux comes from the lens, unless solar type stars are much more likely to host planets of this mass ratio than lower mass stars. We recommend that a method similar to the one developed in this paper be used for other events with high angular resolution follow-up observations when the follow-up observations are insufficient to measure the lens-source relative proper motion., Comment: 35 pages, 7 figures, 6 tables, Accepted for publication in AJ

Published
2017

2. The First Planetary Microlensing Event with Two Microlensed Source Stars

Author

Bennett, D. P., Udalski, A., Han, C., Bond, I. A., Beaulieu, J.-P., Skowron, J., Gaudi, B. S., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Rosenthal, M. M., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yonehara, A., Szymański, M. K., Poleski, R., Soszyński, I., Ulaczyk, K., Wyrzykowski, Ł., DePoy, D., Gould, A., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cole, A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Horne, K., Hundertmark, M., Kains, N., Kane, S. R., Marquette, J.-B., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Zub, M., Bennett, D. P., Udalski, A., Han, C., Bond, I. A., Beaulieu, J.-P., Skowron, J., Gaudi, B. S., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Rosenthal, M. M., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yonehara, A., Szymański, M. K., Poleski, R., Soszyński, I., Ulaczyk, K., Wyrzykowski, Ł., DePoy, D., Gould, A., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cole, A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Horne, K., Hundertmark, M., Kains, N., Kane, S. R., Marquette, J.-B., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., and Zub, M.

Abstract

著者人数: 68名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 小林, 大輔), Accepted: 2018-02-06

Published
2018

3. THE EXTREME MICROLENSING EVENT OGLE-2007-BLG-224: TERRESTRIAL PARALLAX OBSERVATION OF A THICK-DISK BROWN DWARF

Author

Gould, A., Udalski, A., Monard, B., Horne, K., Dong, Subo, Miyake, N., Sahu, K., Bennett, D. P., Wyrzykowski, Ł., Soszyński, I., Szymański, M. K., Kubiak, M., Pietrzyński, G., Szewczyk, O., Ulaczyk, K., Allen, W., Christie, G. W., Depoy, D. L., Gaudi, B. S., Han, C., Lee, C.-U., Mccormick, J., Natusch, T., Park, B.-G., Pogge, R. W., Allan, A., Bode, M. F., Bramich, D. M., Burgdorf, M. J., Dominik, M., Fraser, S. N., Kerins, E., Mottram, C., Snodgrass, C., Steele, I. A., Street, R., Tsapras, Y., Abe, F., Bond, I. A., Botzler, C. S., Fukui, A., Furusawa, K., Hearnshaw, J. B., Itow, Y., Kamiya, K., Kilmartin, P. M., Korpela, A., Lin, W., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagaya, M., Ohnishi, K., Okumura, T., Perrott, Y. C., Rattenbury, N., Saito, To., Sako, T., Skuljan, L., Sullivan, D. J., Sumi, T., Sweatman, W. L., Tristram, P. J., Yock, P. C. M., Albrow, M., Beaulieu, J. P., Coutures, C., Calitz, H., Caldwell, J., Fouqué, P., Martin, Roland, Williams, A., Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astronomical Objects, Solar System, gravitational lensing, Brown dwarf, FOS: Physical sciences, Astrophysics, Gravitational microlensing, 01 natural sciences, law.invention, stars: low-mass, law, 0103 physical sciences, Thick disk, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Lens (optics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astrometry, Astrophysics::Earth and Planetary Astrophysics, Parallax, Event (particle physics), brown dwarfs
Abstract

Parallax is the most fundamental technique to measure distances to astronomical objects. Although terrestrial parallax was pioneered over 2000 years ago by Hipparchus (ca. 140 BCE) to measure the distance to the Moon, the baseline of the Earth is so small that terrestrial parallax can generally only be applied to objects in the Solar System. However, there exists a class of extreme gravitational microlensing events in which the effects of terrestrial parallax can be readily detected and so permit the measurement of the distance, mass, and transverse velocity of the lens. Here we report observations of the first such extreme microlensing event OGLE-2007-BLG-224, from which we infer that the lens is a brown dwarf of mass M=0.056 +- 0.004 Msun, with a distance of 525 +- 40 pc and a transverse velocity of 113 +- 21 km/s. The velocity places the lens in the thick disk, making this the lowest-mass thick-disk brown dwarf detected so far. Follow-up observations may allow one to observe the light from the brown dwarf itself, thus serving as an important constraint for evolutionary models of these objects and potentially opening a new window on sub-stellar objects. The low a priori probability of detecting a thick-disk brown dwarf in this event, when combined with additional evidence from other observations, suggests that old substellar objects may be more common than previously assumed., Comment: ApJ Letters, in press, 15 pages including 2 figures

Published
2009
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5. Microlensing Binaries with Candidate Brown Dwarf Companions

Author

Shin, I.-G., Han, C., Gould, A., Udalski, A., Sumi, T., Dominik, M., Beaulieu, J.-P., Tsapras, Y., Bozza, V., Szymański, M. K., Kubiak, M., Soszyński, I., Pietrzyński, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., The OGLE Collaboration, Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Kobara, S., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Omori, K., Perrott, Y. C., Rattenbury, N., Saito, To., Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., The MOA Collaboration, Christie, G. W., Depoy, D. L., Dong, S., Gal-Yam, A., Gaudi, B. S., Hung, L.-W., Janczak, J., Kaspi, S., Maoz, D., McCormick, J., McGregor, D., Moorhouse, D., Muñoz, J. A., Natusch, T., Nelson, C., Pogge, R. W., Tan, T.-G., Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Malamud, U., Yee, J. C., Choi, J.-Y., Jung, Y.-K., Park, H., Lee, C.-U., Park, B.-G., Koo, J.-R., The μFUN Collaboration, Bajek, D., Bramich, D. M., Browne, P., Horne, K., Ipatov, S., Snodgrass, C., Steele, I., Street, R., Alsubai, K. A., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S., Grundahl, F., Gu, C.-H., Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, Mikkel Nørup, Lundkvist, M., Mancini, L., Mathiasen, M., Hornstrup, A., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, Jesper Fælling, Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Zimmer, F., Albrow, M. D., Batista, V., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cassan, A., Cole, A., Cook, K. H., Corrales, E., Coutures, Ch., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouqué, P., Greenhill, J., Hill, K., Hoffman, M., Kane, S. R., Kubas, D., Marquette, J.-B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Vinter, Christian, and Zub, M.

Subjects
Physics, 010308 nuclear & particles physics, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, gravitational lensing: micro, Astrophysics, Light curve, Gravitational microlensing, 01 natural sciences, Einstein radius, Stars, binaries: general, Settore FIS/05 - Astronomia e Astrofisica, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, brown dwarfs, Parallax, Low Mass, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Brown dwarfs are important objects because they may provide a missing link between stars and planets, two populations that have dramatically different formation history. In this paper, we present the candidate binaries with brown dwarf companions that are found by analyzing binary microlensing events discovered during 2004 - 2011 observation seasons. Based on the low mass ratio criterion of q < 0.2, we found 7 candidate events, including OGLE-2004-BLG-035, OGLE-2004-BLG-039, OGLE-2007-BLG-006, OGLE-2007-BLG-399/MOA-2007-BLG-334, MOA-2011-BLG-104/OGLE-2011-BLG-0172, MOA-2011-BLG-149, and MOA-201-BLG-278/OGLE-2011-BLG-012N. Among them, we are able to confirm that the companions of the lenses of MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149 are brown dwarfs by determining the mass of the lens based on the simultaneous measurement of the Einstein radius and the lens parallax. The measured mass of the brown dwarf companions are (0.02 +/- 0.01) M_Sun and (0.019 +/- 0.002) M_Sun for MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149, respectively, and both companions are orbiting low mass M dwarf host stars. More microlensing brown dwarfs are expected to be detected as the number of lensing events with well covered light curves increases with new generation searches., 10 pages, 9 figures, 4 tables

Published
2012
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6. OGLE-2005-BLG-071Lb, the Most Massive M Dwarf Planetary Companion?

Author

Dong, Subo, Gould, Andrew, Udalski, Andrzej, Anderson, Jay, Christie, G. W., Gaudi, B. S., The OGLE Collaboration, Jaroszyński, M., Kubiak, M., Szymański, M. K., Pietrzyński, G., Soszyński, I., Szewczyk, O., Ulaczyk, K., Wyrzykowski, Ł., The ΜFUN Collaboration, DePoy, D. L., Fox, D. B., Gal-Yam, A., Han, C., Lépine, S., McCormick, J., Ofek, E., Park, B.-G., Pogge, R. W., The MOA Collaboration, Abe, F., Bennett, D. P., Bond, I. A., Britton, T. R., Gilmore, A. C., Hearnshaw, J. B., Itow, Y., Kamiya, K., Kilmartin, P. M., Korpela, A., Masuda, K., Matsubara, Y., Motomura, M., Muraki, Y., Nakamura, S., Ohnishi, K., Okada, C., Rattenbury, N., Saito, To., Sako, T., Sasaki, M., Sullivan, D., Sumi, T., Tristram, P. J., Yanagisawa, T., Yock, P. C. M., Yoshoika, T., The PLANET/Robo Net Collaborations, Albrow, M. D., Beaulieu, J. P., Brillant, S., Calitz, H., Cassan, A., Cook, K. H., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Hill, K., Hoffman, M., Horne, K., Jørgensen, U. G., Kane, S., Kubas, D., Marquette, J. B., Martin, Roland, Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Vinter, C., Wambsganss, J., Williams, A., Bode, M., Bramich, D. M., Burgdorf, M., Snodgrass, C., Steele, I., Doublier, Vanessa, Foellmi, Cedric, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Astronomische Rechen-Institut [Heidelberg] (ARI), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg]-Universität Heidelberg [Heidelberg], Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg] = Heidelberg University-Universität Heidelberg [Heidelberg] = Heidelberg University, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
gravitational lensing, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gravitational microlensing, 01 natural sciences, Jovian, Galaxy: bulge, Neptune, Primary (astronomy), Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Planetary system, Light curve, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Planetary mass
Abstract

We combine all available information to constrain the nature of OGLE-2005-BLG-071Lb, the second planet discovered by microlensing and the first in a high-magnification event. These include photometric and astrometric measurements from Hubble Space Telescope, as well as constraints from higher order effects extracted from the ground-based light curve, such as microlens parallax, planetary orbital motion and finite-source effects. Our primary analysis leads to the conclusion that the host of Jovian planet OGLE-2005-BLG-071Lb is an M dwarf in the foreground disk with mass M= 0.46 +/- 0.04 Msun, distance D_l = 3.3 +/- 0.4 kpc, and thick-disk kinematics v_LSR ~ 103 km/s. From the best-fit model, the planet has mass M_p = 3.8 +/- 0.4 M_Jup, lies at a projected separation r_perp = 3.6 +/- 0.2 AU from its host and so has an equilibrium temperature of T ~ 55 K, i.e., similar to Neptune. A degenerate model less favored by \Delta\chi^2 = 2.1 (or 2.2, depending on the sign of the impact parameter) gives similar planetary mass M_p = 3.4 +/- 0.4 M_Jup with a smaller projected separation, r_\perp = 2.1 +/- 0.1 AU, and higher equilibrium temperature T ~ 71 K. These results from the primary analysis suggest that OGLE-2005-BLG-071Lb is likely to be the most massive planet yet discovered that is hosted by an M dwarf. However, the formation of such high-mass planetary companions in the outer regions of M-dwarf planetary systems is predicted to be unlikely within the core-accretion scenario. There are a number of caveats to this primary analysis, which assumes (based on real but limited evidence) that the unlensed light coincident with the source is actually due to the lens, that is, the planetary host. However, these caveats could mostly be resolved by a single astrometric measurement a few years after the event., Comment: 51 pages, 12 figures, 3 tables, Published in ApJ

Published
2009
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8. EXTREME MAGNIFICATION MICROLENSING EVENT OGLE-2008-BLG-279: STRONG LIMITS ON PLANETARY COMPANIONS TO THE LENS STAR

Author

Yee, J. C., primary, Udalski, A., additional, Sumi, T., additional, Dong, Subo, additional, Kozłowski, S., additional, Bird, J. C., additional, Cole, A., additional, Higgins, D., additional, McCormick, J., additional, Monard, L. A. G., additional, Polishook, D., additional, Shporer, A., additional, Spector, O., additional, Szymański, M. K., additional, Kubiak, M., additional, Pietrzyński, G., additional, Soszyński, I., additional, Szewczyk, O., additional, Ulaczyk, K., additional, Wyrzykowski, Ł., additional, Poleski, R., additional, Allen, W., additional, Bos, M., additional, Christie, G. W., additional, DePoy, D. L., additional, Eastman, J. D., additional, Gaudi, B. S., additional, Gould, A., additional, Han, C., additional, Kaspi, S., additional, Lee, C. -U., additional, Mallia, F., additional, Maury, A., additional, Maoz, D., additional, Natusch, T., additional, Park, B. -G., additional, Pogge, R. W., additional, Santallo, R., additional, Abe, F., additional, Bond, I. A., additional, Fukui, A., additional, Furusawa, K., additional, Hearnshaw, J. B., additional, Hosaka, S., additional, Itow, Y., additional, Kamiya, K., additional, Korpela, A. V., additional, Kilmartin, P. M., additional, Lin, W., additional, Ling, C. H., additional, Makita, S., additional, Masuda, K., additional, Matsubara, Y., additional, Miyake, N., additional, Muraki, Y., additional, Nagaya, M., additional, Nishimoto, K., additional, Ohnishi, K., additional, Perrott, Y. C., additional, Rattenbury, N. J., additional, Sako, T., additional, Saito, To., additional, Skuljan, L., additional, Sullivan, D. J., additional, Sweatman, W. L., additional, Tristram, P. J., additional, Yock, P. C. M., additional, Albrow, M. D., additional, Batista, V., additional, Fouqué, P., additional, Beaulieu, J. -P., additional, Bennett, D. P., additional, Cassan, A., additional, Comparat, J., additional, Coutures, C., additional, Dieters, S., additional, Greenhill, J., additional, Horne, K., additional, Kains, N., additional, Kubas, D., additional, Martin, R., additional, Menzies, J., additional, Wambsganss, J., additional, Williams, A., additional, and Zub, M., additional

Published
2009
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9. A Low‐Mass Planet with a Possible Sub‐Stellar‐Mass Host in Microlensing Event MOA‐2007‐BLG‐192

Author

Bennett, D. P., primary, Bond, I. A., additional, Udalski, A., additional, Sumi, T., additional, Abe, F., additional, Fukui, A., additional, Furusawa, K., additional, Hearnshaw, J. B., additional, Holderness, S., additional, Itow, Y., additional, Kamiya, K., additional, Korpela, A. V., additional, Kilmartin, P. M., additional, Lin, W., additional, Ling, C. H., additional, Masuda, K., additional, Matsubara, Y., additional, Miyake, N., additional, Muraki, Y., additional, Nagaya, M., additional, Okumura, T., additional, Ohnishi, K., additional, Perrott, Y. C., additional, Rattenbury, N. J., additional, Sako, T., additional, Saito, To., additional, Sato, S., additional, Skuljan, L., additional, Sullivan, D. J., additional, Sweatman, W. L., additional, Tristram, P. J., additional, Yock, P. C. M., additional, Kubiak, M., additional, Szymański, M. K., additional, Pietrzyński, G., additional, Soszyński, I., additional, Szewczyk, O., additional, Wyrzykowski, Ł., additional, Ulaczyk, K., additional, Batista, V., additional, Beaulieu, J. P., additional, Brillant, S., additional, Cassan, A., additional, Fouqué, P., additional, Kervella, P., additional, Kubas, D., additional, and Marquette, J. B., additional

Published
2008
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